ESA's Holland-Area Exoplanet Science Meeting (HAESM) 2026

Uniting all ESA and Holland-area exoplaneteers for a day of science, discussions, and collaboration; our colleagues from ESAC, STScI, and external institutions are equally encouraged to join us remotely.
Tuesday, 7 April 2026, 12:55 - 18:00 CEST, in ESTEC and online (via WebEx).​​​​​​

Programme

Given the high subscription this year, we will use this as an opportunity to experiment with a slightly different format. Science presentations will remain at 10 minutes (talking time). But instead of questions after each presentation, we will schedule a shared window for high-level science questions to all speakers at the end of the session, followed by an extended coffee break where people can touch base with more detailed detail-level technical questions and use this as an opportunity to network and start collaborating. HAESM 2026 seeks to give everyone a platform to present their work, and especially encourages contributions from early career scientists. The event also actively encourages any and all "unconference" approaches, and as such is also open to submissions of ideas for group discussions, brainstormings, diversity workshops, and other events that fit the scope. 

Local information

Arrival and social programme: All in-person attendees are invited to arrive at the ESTEC security gatehouse (Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands) at 11:00 CEST. You must bring your passport with you to collect your scientific visitor badges for the day. You can reach ESTEC by bicycle or local bus systems (e.g. from Leiden Centraal); for your individual travel planning please consult an online map service. Our colleagues from security and our friendly helpers will receive you and guide you from there to our ESTEC cafeteria, where we can enjoy a coffee and lunch (self-paid). The science programme starts from 12:55 CEST, with a mix of in-person and virtual presentations. Of course, we have planned for ample room for networking and exchange during two complementary coffee breaks. Finally, we hope to enjoy a relaxing evening in the Dutch Sun and continue with informal science discussions during a borrel at the ESCAPE lounge from around 18:00 CEST.

Meeting rooms: We have booked a group of our most modern meeting rooms, surrounding our complementary coffee corner. No worries, we will guide you there. Given the group size (and to inspire a touch of healthy competition?), we’ll split into two or three teams across the large rooms. The smaller rooms will also be available for direct tag-ups and collaborative chats between participants. All rooms have glass walls, so you can still wave at your colleagues across the hall. For reference, these are called Land 1, Land 2, Ocean 1, and (you guessed it) Ocean 2.

WebEx: The meeting and all presentations will happen in WebEx. If you are not familiar with WebEx, please ask for a short test session before the meeting starts. If it is your first time using WebEx, you will usually have to adjust a couple of system settings and restart the software or your whole computer. The WebEx link is shared via email.

Abstracts

More observing opportunities with CHEOPS
The CHaracterising ExOPlanet Satellite (CHEOPS) is providing precise, space-based photometry of known exoplanets, yielding high-accuracy radius measurements and key insights into planetary densities, compositions, and system architectures. These results inform how planetary properties relate to their host stars and environments—central themes in understanding the role of stellar and Galactic context in planet formation and evolution. We announce the upcoming new opportunities to observe with CHEOPS as part of a new Running Call, which will start in 2026, contingent on mission extension, and summarise the mission’s major scientific contributions to date. These include refinement of planet radii across diverse populations, detection of transit timing and phase-curve effects, and targeted follow-up of objects identified by ground- and space-based surveys. A practical overview of the Running Call will guide prospective applicants through the proposal process, highlighting web-based planning tools that require no local software installation and facilitate feasibility assessment and observation design. Finally, we discuss synergies between CHEOPS and ESA’s PLATO mission in the context of exoplanet science: CHEOPS’ targeted follow-up can refine parameters and ephemerides for PLATO’s wide-field discoveries, enhancing demographic studies across different stellar populations and Galactic environments.

New mass constraints on circumbinary planets: Kepler-38 b and Kepler-1647 b
Circumbinary planets (CBPs), planets orbiting binary star systems, offer unique insights into planet formation. However, they are challenging to detect using traditional methods. While photometric surveys such as Kepler and TESS have led to the discovery of around a dozen transiting CBPs, the majority of these systems lack precise mass measurements due to limitations of transit-based methods. Radial velocity (RV) observations provide a direct way to measure planetary masses and detect non-transiting CBPs. Two circumbinary planets with some of the largest uncertainties on planet mass from the known catalogue are Kepler-38b - an <122 Earth Mass planet orbiting an 18.8d binary, and Kepler-1647b - an 483±206 Earth Mass planet orbiting an 11.3d binary. Kepler-1647b is notable for its unusually wide 1108-day orbit beyond the stability limit. In this talk I will present an analysis of CARMENES RV data of these faint targets (V~13.5) to establish detection limits for additional planets, and update mass constraints using a full photodynamical fit.

Automated Transit Signal Detection in CHEOPS Observations Using Machine Learning
The CHaracterising ExOPlanet Satellite (CHEOPS) enables high-precision photometry of known exoplanet host stars, allowing refined measurements of planetary radii and compositions. However, the CHEOPS Data Reduction Pipeline (DRP) produces lightcurves using multiple photometric apertures that differ in their sensitivity to background contamination, instrumental systematics, and stellar variability, leading to heterogeneous noise properties across visit-based observations and increasing the complexity and time required for reliable transit signal identification. This project develops a reproducible machine learning framework to classify CHEOPS visit-level lightcurves as Transit or No-Transit without relying on prior ephemerides. To construct the labeled dataset, more than 7000 lightcurve images across different noise regimes were visually inspected and assigned labels, followed by exploratory data analysis to validate label consistency and characterize the statistical properties of the observations. Multiple baseline Random Forest modeling strategies were explored using statistical descriptors and flux-based representations of the lightcurves. Feature importance analysis guided feature selection prior to training the final model. The best-performing model, based on statistical descriptors, achieved an accuracy of 0.90 and an AUC of 0.96 on the test set, with balanced precision and recall for both Transit and No-Transit classes. Injection–recovery experiments were further performed to construct sensitivity maps of transit detectability as a function of signal depth and photometric noise, providing an empirical characterization of the model’s detection limits across heterogeneous CHEOPS observations. Our project generated a robust data-driven method to select the optimal DRP apertures to use for any CHEOPS single visit observation and can be used by CHEOPS observers to simplify/accelerate their data analysis.

Space-based exoplanet imaging with vector vortex coronagraphs
The Habitable Worlds Observatory promises to detect rocky planets in the habitable zones of nearby stars and search for biosignatures in their atmospheres. One of the most critical components to achieve this ambitious goal is the coronagraph. In this talk, I will present the results of the ESA-funded SUPPPPRESS project, which brings together a European consortium to mature and demonstrate liquid-crystal polymer based vortex coronagraphs. I will discuss the big improvements in manufacturing quality we have made at Colorlink Japan and show that we can currently reach raw contrasts of 2 x 10^-8 for monochromatic light and 6x10^-8 in 10% bandwidth. Finally, I will discuss future plans and the applicability of the same technology to other exoplanet related missions.

Highly eccentric but aligned warm Jupiter around the 9 Gyrs old star TIC61024636
Warm Jupiters are Jupiter-sized planets with orbital periods between 10 and 200 days. Unlike hot Jupiters, they orbit further from their host stars and are therefore subject to less extreme irradiation environments. As a result, their orbital architectures could retain dynamical signatures and help distinguish between formation pathways ranging from disk-driven migration and in situ formation to dynamical processes such as planet–planet scattering. In this work, we characterise a newly discovered warm Jupiter around the 9 Gyr old star TIC61024636. We employ the juliet framework to jointly model the TESS and NGTS photometry and CORALIE radial velocities and constrain the orbital and planetary parameters of the system. Additionally, we use ironman to model the ESPRESSO data taken during one planetary transit to detect the Rossiter-McLaughlin effect and probe the spin-orbit architecture of the system. Our analysis reveals that TIC61024636 is hosting a highly eccentric (e = 0.7) and massive (5 Mjup) warm Jupiter on an aligned orbit. This configuration poses strong constraints on the possible migration scenarios and provides new insight into the dynamical histories of the warm Jupiter population.

Exoplanets in the Evolving Stellar Environment
In recent years the feasibility of life emerging on planets orbiting M dwarfs have come under ever increasing scrutiny. It became commonly accepted that for abiogenesis to occur on the surface, a planet needs a large magnetosphere in order to protect it from the highly energetic stellar environment. For a a bow shock to form, a planet needs to orbit in the super-Alfvénic regime of the stellar wind, but studies showed that certain planets orbit in the sub-Alfvénic regime where the star and planet can connect magnetically leading to different nature of star-planet interactions. Can exoplanets truly be classified into one of these two regimes or can stellar activity cycles make them oscillate in between the two? The goal of this talk is to describe the analysis of the evolution of the stellar environment around a sample of seven M dwarfs, including exoplanet-hosting stars. I will present a set of new stellar wind simulations associated to maps of the magnetic field reconstructed over a few months. To gain a more comprehensive view of the variability of stellar magnetism, I will also compare the simultaneous changes in large and small scale magnetic fields. I will conclude by discussing the impact of my results on the confirmed exoplanets around some of these stars.

The spectral energy distribution of YSES 1 b and its circumplanetary disk
YSES 1 b is a directly imaged young substellar companion on a wide orbit of 160 AU, making it an interesting challenge for formation theories. Initial photometric observations with SPHERE and NACO from Y to M band suggested physical parameters of Teff=1700 K, R=3 R_J and M=14 M_J. Here, we present new observations in the r’, i’ and z’ band using the MagAO-X instrument and revisit the modelling of YSES 1 b based on the combined MagAO-X, SPHERE and NACO data. In addition, we update the forward model by including the effect of possible dust extinction from the circumplanetary disk (CPD) which was recently confirmed with JWST.  The newly derived parameters result in a higher Teff of 2800 K and a more physically expected radius of 1.6 R_J. The mass increases to 26 or 42 M_J, depending on the age used for the system. This result suggests that YSES 1 b resides more in the brown dwarf realm rather than the planetary regime.

Silicate clouds: Drivers of variability in the emission of lava worlds
55 Cnc e is the first rocky exoplanet for which strong evidence of a thick, volatile atmosphere exists (Hu+2024). The  atmosphere of this hot super Earth shows sub weekly variability in emission (Demory+2016, Meier-Valdez+2023, Patel+2024). Among the multiple suggested  scenarios is an outgassing – cloud formation cycle driving this variability.  We investigate, whether lava worlds could host variable, cloudy atmospheres utilizing a 1D, non time varying approach.  We construct a pipeline which combines radiative transfer with equilibrium chemistry, a cloud formation model (ARCiS, Min+2020) and outgassing of the magma (LavAtmos 2.0, vanBuchem+2025). We run this setup for a selection of atmospheric compositions and surface pressures for the purpose of our investigation and estimate the duration of each stage in the cycle from the physical processed involved. In this talk I will present the results of this study, focusing on the spectral variability on  cloudy lava worlds and their timescales.

Imaging rocky exoplanets with the Extremely Large Telescope's Planetary Camera and Spectrograph
The Planetary Camera and Spectrograph (PCS) will be the ELT’s dedicated instrument for exoplanet characterization, with a central goal of discovering and studying rocky exoplanets. To prepare for these ambitious objectives, the PCS R&D consortium, launched in January 2025 under ESO’s leadership, was established to advance the conceptual design and bridge critical technology gaps. I will present an overview of the scientific goals of the instrument and the technology that we are developing. The Dutch astronomical community through NOVA is aiming to become a large partner of the PCS instrument. I will discuss how we are involved and how the community can join the effort.

Planet-like or star-like? The puzzling nature of magnetic fields in ultracool dwarfs
H-alpha emission is abundant in ultracool dwarfs (UCD), but its origin is unclear. It may stem from residual star-like, chromospheric emission, but could also be attributed to planet-like magnetospheric emission akin to Jupiter's aurora. The spatial distribution of H-alpha emission on the UCD can resolve this ambiguity: Chromospheric emission would appear distributed in spots, and/or spread out across the entire surface. In contrast, auroral emission would manifest as a ring structure centered on the magnetic axis, produced by particles precipitating along a largely dipolar magnetosphere. In this talk, I will present the first application of this method using time series of high-resolution spectra of LSR J1835, a young nearby brown dwarf. I will show evidence that the H-alpha emission from LSR J1835 emanates from a combination of an oblique ring with several high-latitude spots, suggesting that the UCD produces a chimera: a residual stellar chromosphere, embedded in a largely dipolar magnetosphere powering the auroral ring. This is consistent with the broader observational record of LSR J1835, which shows both planet-like features like radiation belts and coherent emission at radio frequencies, and star-like flares in its optical photometry. Finally, I will demonstrate that discriminating different emission structures through forward modeling and Bayesian analysis is possible, but requires high signal-to-noise, high-resolution spectra that place LSR J1835 as the only viable target. However, looking ahead, ELT/ANDES will extend our reach to spectral types as late as L3, opening a new window into the magnetic and atmospheric physics of UCDs, and the space weather of planets around them.

Results from the WIde Separation Planets In Time (WISPIT) survey
The WIde Separation Planets In Time (WISPIT) survey is a VLT/SPHERE snapshot survey that targets 178 solar-mass stars with ages ranging from <5 to 20 Myr spanning the entire sky observable by VLT. Its goal is to detect and characterize wide-separation planetary mass companions. Published discoveries from this survey are the WISPIT 1 system and, most notably, the WISPIT 2 system. WISPIT 1 is a ~16 Myr binary with a solar-type primary that hosts a ~10 Jupiter mass and ~5 Jupiter mass companion at separations of 338 au and 840 au, respectively, making it among the widest separation directly imaged planets to date. WISPIT 2 is another multi-planet system; this ~5 Myr version of our sun hosts a spectacular multi-ringed disk with two embedded planets. The discovery of WISPIT 2b marked the first unambiguous detection of a gap-carving embedded planet, and with the recent spectroscopic confirmation of the second planet WISPIT 2c, this will likely be a benchmark system for models of planet formation and planet-disk interactions for years to come. Both the WISPIT 1 and WISPIT 2 systems are novel and unexpected in their own way, and not only revealed new planets but also redefined where we should search for planets and how future direct imaging surveys should be designed.

What JWST Really Sees: Time-Dependent Atmospheric Signatures
The interpretation of exoplanet spectra obtained with JWST typically assumes that observed atmospheres are in steady state. In this work, we challenge that assumption by demonstrating that stellar flares can induce rapid and long-lasting changes in atmospheric composition that directly impact observables. We model the effects of recurrent stellar flaring on metal-rich exoplanet atmospheres using time-dependent photochemistry and radiative transfer. We find that flare activity drives strong variability in key molecules such as SO₂, CO₂, CH₄, and H₂O, producing spectral changes at the tens to hundreds of parts-per-million level, well within JWST sensitivity. Extreme flares can temporarily suppress molecular features, while cumulative flaring leads to persistent compositional shifts on decadal timescales. These results imply that JWST spectra do not necessarily probe a planet’s equilibrium state, but rather a snapshot conditioned on recent stellar activity. Atmospheric retrievals must therefore account for temporal variability to avoid biased inferences of composition and climate, especially for planets orbiting active stars.

Leveraging long-term spectroscopy surveys: A fast technique to measure relative small-scale magnetic field variations
Magnetic fields are a key ingredient in our understanding of stars and planets: they play a crucial role in their formation, drive stellar activity phenomena, and induce spurious signals in exoplanet datasets, in particular in radial velocity (RV) measurements. Characterizing the variability of magnetic fields in M dwarfs is especially important, as these stars are prime targets in the search for Earth-like exoplanets. Direct modeling of stellar spectra enables measurements of the total magnetic field at the stellar surface, about 90% of which is typically associated with small-scale magnetic fields operating in localized regions of the stellar surface (spots and plages). In this talk, I present a newly proposed method to derive relative variations of small-scale magnetic fields from time series of high-resolution spectra. Using near-infrared spectra collected over several years, we measure surface magnetic fields for each observing night. In addition to providing clear constraints on stellar rotation periods, the derived magnetic field measurements are strongly anti-correlated with surface temperature variations, suggesting that the M dwarfs in our sample host heavily spotted stellar surfaces. On longer timescales, the observed variations in magnetic field strength point to significant changes in the fraction of the stellar surface covered by magnetic features, which could be associated with magnetic cycles. Our method allows one to derive fast and reliable magnetic field estimates directly from the spectra used to measure RVs. These kind of measurements pave the way to future studies by offering constraints on the behavior of stellar magnetic fields, and data which can be used to correct RV curves used for exoplanet detection. These developments are especially relevant for current and future high-precision spectroscopic facilities such as WINERED (Magellan-Clay), WENAOKEAO (CFHT), and ANDES (ELT).

Photometric characterization of starspots on exoplanet host stars
With growing interest in exoplanet characterization, the importance of studying starspots has become increasingly evident, as they can obscure or mimic planetary atmospheric signals in transmission spectroscopy. Understanding their properties (e.g., temperature, size, and distribution) is essential for properly accounting for these effects. In this context, we have conducted photometric observations of stellar rotational modulation and spot-crossing transits for several key exoplanet host stars, using the LCO 1m telescopes with Sinistro and the multi-band MuSCAT instruments. Our study demonstrates that multi-band photometry of stellar rotational modulation, especially when combined with spot-crossing transits, is a powerful approach to break degeneracies in spot mapping, particularly for parameters such as spot size and temperature. Such observations, when carried out contemporaneously with transmission spectroscopy from facilities such as JWST and Ariel, provide crucial auxiliary data for robust detections of planetary atmospheres. In this presentation, we will introduce our study of the TOI-3884 system and present recent results applying this method to young exoplanet host stars.

From Gas to Clouds: Investigating FeH in Brown Dwarf Atmospheres
At the transition between spectral types L and T, brown dwarfs are characterized by their pronounced variability, brighter J-band fluxes, and bluer near-infrared colours. The cloud-clearing hypothesis has been proposed as the leading explanation for these features, as well as for the re-emergence of FeH absorption in the spectra of early- to mid-T dwarfs. FeH is therefore a promising tracer of cloud evolution across the L/T transition. In this work, I investigate the presence of FeH in a diverse sample of young brown dwarfs, using medium-resolution spectra observed as part of the X-SHYNE survey. Applying cross-correlation techniques, I find that the FeH signal is strongest in early- to mid-L dwarfs, it weakens toward late-L and T types, but remains detectable in early-T atmospheres. These findings support current interpretations in which FeH traces the changing cloud coverage of brown dwarf atmospheres through the L/T transition.

Ariel and JWST synergies for exoplanets
I will present a white paper exploring the potential for strategic synergies between the JWST and the Ariel telescopes. Both telescopes have the potential to address common fundamental questions about exoplanets-especially concerning their nature and origins-and serve a growing scientific community. With their operations now anticipated to overlap, starting from 2030, there is a unique opportunity to enhance the scientific outputs of both observatories through coordinated efforts. In this report, authored by the Ariel-JWST Synergy Working Group, we summarise the capabilities of JWST and Ariel; we highlight their key differences, similarities, synergies, and distinctive strengths. This presentation will discuss key pathways for fostering JWST-Ariel synergies, many of which can be initiated even before Ariel's launch. Leveraging their complementary designs and scopes, JWST and Ariel can jointly address fundamental questions about the nature, formation, and evolution of exoplanets. Such strategic collaboration has the potential to maximise the scientific returns of both observatories and lay the foundation for future facilities in the roadmap to exoplanet exploration.

Star-planet magnetic interactions in photoevaporating exoplanets
Star-planet magnetic interactions (SPMI) arise when a close-in exoplanet is magnetically connected to its host star. In this scenario, the energy fluxes arising from the interaction can power enhanced emission in the stellar chromosphere. By comparing the power inferred from observations of stellar chromospheric lines with analytical theories of SPMI, it is possible to place constraints on the magnetic field strength of the planet. Analytical SPMI models are usually adapted from the moon-planet magnetic coupling observed in the Solar System. However, these analytical models typically underpredict the energy inferred from observations of exoplanetary systems. Unlike moons, many close-in exoplanets are extended, gaseous bodies subject to intense stellar irradiation that drives atmospheric evaporation. While both atmospheric escape and SPMI have been studied separately, it is not known how these two forms of star-planet interaction influence one another. In this work, we present three-dimensional radiation, magneto-hydrodynamic simulations that model planetary evaporation and SPMI simultaneously for the first time. Our results show that, when atmospheric escape is included, the SPMI power can increase by more than an order of magnitude compared with standard analytical estimates. We derive a scaling law that incorporates atmospheric evaporation, which can be used to predict SPMI energetics from photoevaporating planets. This results offers a practical method to better constrain exoplanetary magnetism from SPMI observations.

Exploring a Gaussian Process Framework for Modelling CHEOPS Systematics and Stellar Variability
The CHEOPS mission (CHaracterising ExOPlanet Satellite) provides high precision optical photometry for the follow-up and characterisation of exoplanet candidates. The CHEOPS raw lightcurves exhibit well-characterised instrumental systematics arising from spacecraft operations, particularly roll-angle-dependent variations. The current Data Reduction Pipeline (DRP) is designed to mitigate these effects for the majority of science cases and research teams often apply additional post-processing steps tailored to their specific science objectives. Applying different approached however may lead to differences in results across datasets and, in some cases, may limit the extent to which intrinsic astrophysical signals are preserved alongside planetary transits. In this work, we explore a Gaussian Process (GP)-based framework to model and separate instrumental systematics from astrophysical variability in CHEOPS lightcurves. The approach treats the observed flux as the sum of a time-dependent component, capturing stellar variability and long-term trends, and a roll-angle-dependent component, accounting for spacecraft-induced systematics. By applying this model to a diverse sample of CHEOPS observations, we aim to assess its ability to disentangle these signals in a consistent way. The broader goal is to develop a standardised, agnostic detrending method that can be applied uniformly across the CHEOPS archive. While the resulting precision may not be sufficient for detailed planet characterisation studies, such a framework would enable robust population-level and survey analysis by producing comparable lightcurves across targets. The final pipeline is envisioned to be utilised by existing platforms, such as ESASky and ESA Datalabs, while it can also be leveraged for citizen science initiatives. This work is ongoing, and we invite discussion on potential applications and integration with community tools.

Stellar Flares as probes of Exoplanet Atmospheres and Star-Planet Interaction
Stellar flares are strong magnetic events that can affect the atmospheres of nearby orbiting planets. These events can be very disruptive and influence atmospheric escape, but can also trigger the chemical conditions relevant for prebiotic chemistry. Understanding these effects requires reliable estimates of flare energies. In this work, we study flares from a highly active star observed with both TESS and ASTEP, a telescope located in Antarctica that provides dual-band photometry. These observations allow us to estimate flare temperatures and obtain more realistic flare energies than the commonly adopted assumption of a constant temperature in the literature. These improved estimates help to better characterise the high-energy environment that close-in planets may experience. Since these planets also influence stellar magnetic activity and may trigger flares, we investigate whether patterns in the flare occurrence could indicate the presence of close-in planets, exploring flares as a potential indirect signature of star-planet interaction.

CHEOPS observations of V1298 Tau: improved planetary densities and implications on the early evolution of the young system
The young (10-30 Myr) multi-planet system V1298 Tau presents a unique opportunity to probe the early formation and evolution of young systems. However, precise measurements of planetary masses and radii are challenging due to the high stellar activity of the host star. We present new CHEOPS observations of the three innermost planets, yielding high-precision planetary radii (~5-11 Re) and improving the radius ratios (Rp/Rs) by 30-71%. Combined with refined period and mass determinations from transit-timing variation (TTV) measurements, we derive updated bulk densities for these planets ranging between 0.23-0.06 g/cm3 from the innermost to the outermost planet. We find evidence that the innermost planet is ∼3 times more dense than the second innermost planet at a 3.4 sigma level. The higher density of the innermost planet may indicate enhanced atmospheric escape, which reflects differential atmospheric evolution in the system. We additionally explore the dynamical state of the system and find no evidence that the system is trapped in a mean-motion resonance (MMR). The low eccentricities and the normalised angular momentum deficit (NAMD) of the system point to a dynamically quiescent configuration. Our refined planetary radii allows for a more precise tidal evolution analysis that previously done for this system. We find that the tidal migration will only have a minor impact on the architecture of the system as expected given its young age.

Stellar Activity Photometric Monitoring for Transmission Spectroscopy with the SPACE Program
The importance of understanding stellar activity has been growing as the precision of transmission spectroscopy improves. Host star spots and faculae can hinder planetary atmosphere retrieval, and flares might even shape the planetary atmospheres. The SPACE Program (PI: L. Kreidberg) is an HST program aiming at characterizing the atmospheres of eight sub-Neptunes. To investigate the impact of stellar activity, we photometrically monitored the host stars from 2022 to 2024 with the automated 0.6-m telescope at Wesleyan University (Connecticut, USA). For some targets, we confirm no variability beyond the instrument precision; for others that exhibit variations, we propose connections between photometry and measured transit parameters. We demonstrate that the unique combination of a moderately long baseline and high precision can enhance the analysis of transmission spectra and facilitate the characterization of exoplanet atmospheres.

Registration and abstract submission (Deadline: Friday, 27 March 2026)

Registration and abstract submission have closed on Friday, 27 March, and the programme has been announced here on Tuesday, 31 March.

ESA Member States and Cooperating States

To review which countries are ESA Member States and Cooperating States, and to access the most up‑to‑date overview of their participation, you can consult the current list here.

Personal Data Protection

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The European Space Agency (ESA) strives to create a positive work environment where all people are treated with respect and dignity. In the context of ESA Science workshops and conferences, all participants are expected to help create an environment at the meeting and all associated activities that is professional, inclusive, and in which everyone is treated with respect.

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Acknowledgments: This code of conduct has been adapted from the London Code of Conduct (by A. Pontzen and H. Peiris), which was derived from original Creative Commons documents by PyCon and Geek Feminism. It is released under a CC-Zero licence for reuse. To help track people's improvements and best practice, please retain this acknowledgement, and log your re-use or modification of this policy at: https://github.com/apontzen/london_cc .

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